Modeling pulsar pole emissions as two Gaussian beams, a core and a cone, enables us to constrain the viewing geometry of millisecond pulsars and estimate their magnetic inclination and impact angles. We fit the profiles of millisecond pulsars found on the European Pulsar Network database. When good polarization data is available we also fit the position angle sweeps of the millisecond pulsars using the rotation vector model, allowing us to find the maximum rate of position angle sweep. We can then constrain the magnetic inclination in order to determine the impact angle. Fitting these pulsars for multiple frequencies allows us to more accurately estimate the viewing geometry. We can then incorporate the beam geometry into pulsar population models and determine the number of observable and unobservable pulsars.